Coronal Turbulence Driven from the Sun's Photosphere: Preparing for the Era of the Daniel K. Inouye Solar Telescope

太阳物理学中尚未解决的主要问题之一是太阳日冕如何被加热到100多万度的温度。一种被怀疑的机制是，太阳表面附近的磁场能量通过波和湍流的耗散转化为热能。在这个提案中，PI将开发磁流体动力学（MHD）波和湍流的数值模型。这些模型将使PI能够追踪这些特征从太阳表面向外传播到外日冕时的动态演变。数值模拟将做出预测，这些预测可以通过Daniel K. Inouye太阳望远镜（DKIST）等望远镜进行的高分辨率观测来验证。拟议的研究将支持下一代太阳科学家的培训。该项目将涉及一名研究生，并计划将研究纳入他的本科和研究生课程。在这个提议中，PI提议建立一个现实的，基于物理的MHD波动模型，从太阳出发？太阳表面进入外日冕以阐明日冕加热的问题。根据目前的观测，微小的、颗粒间的、磁通量浓度的动力学一直很困难，然而，这些结构形成了最终将日冕加热到如此高温度的种子。PI将产生的模型将用于跟踪颗粒间磁通量元素，并测量它们向外移动到日冕时的演变。然后，这些模型将用于为DKIST等望远镜生成可观测诊断，以测试MHD湍流理论。

One of the major unsolved problems in solar physics is the question regarding how the solar corona is heated to temperatures over a million degrees. One suspected mechanism is the conversion of magnetic field energy near the Sun's surface into heat energy through the dissipation of waves and turbulence. In this proposal, the PI will develop numerical models of magnetohydrodynamic (MHD) waves and turbulence. These models will allow the PI to trace the dynamical evolution of these features as they travel outward from the surface of the Sun into the outer corona. The numerical simulations will make predictions that can be tested by high-resolution observations made by telescopes such as the Daniel K. Inouye Solar Telescope (DKIST). The proposed research will support the training of the next generation of solar scientists. The PI will involve a graduate student in the proposed work and also plans to incorporate the research into his undergraduate and graduate courses. In this proposal, the PI proposes to construct realistic, physics-based models of MHD fluctuations traveling from the Sun?s surface into the outer corona to shed light on the problem of coronal heating. With current observations, the dynamics of small, inter-granular, magnetic flux concentrations have been difficult, however, these structures form the seeds that eventually heat the corona to such high temperatures. The models that the PI will produce will be used to track the inter-granular magnetic flux elements and measure their evolution as they move outward into the corona. The models will then be used to generate observable diagnostics for telescopes like DKIST to test the MHD turbulence theory.